EMPRESS. XIII. Chemical Enrichment of Young Galaxies Near and Far at z ∼ 0 and 4–10: Fe/O, Ar/O, S/O, and N/O Measurements with a Comparison of Chemical Evolution Models

We present gas-phase elemental abundance ratios of thirteen local extremely metal-poor galaxies (EMPGs), including our new Keck/LRIS spectroscopy determinations together with 33 James Webb Space Telescope z ∼ 4–10 star-forming galaxies in the literature, and compare chemical evolution models. We dev...
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Autor*in:	Kuria Watanabe [verfasserIn] Masami Ouchi [verfasserIn] Kimihiko Nakajima [verfasserIn] Yuki Isobe [verfasserIn] Nozomu Tominaga [verfasserIn] Akihiro Suzuki [verfasserIn] Miho N. Ishigaki [verfasserIn] Ken’ichi Nomoto [verfasserIn] Koh Takahashi [verfasserIn] Yuichi Harikane [verfasserIn] Shun Hatano [verfasserIn] Haruka Kusakabe [verfasserIn] Takashi J. Moriya [verfasserIn] Moka Nishigaki [verfasserIn] Yoshiaki Ono [verfasserIn] Masato Onodera [verfasserIn] Yuma Sugahara [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2024

Schlagwörter:	Galaxy chemical evolution Galaxy evolution Chemical enrichment Chemical abundances Galaxy formation Sculptor dwarf elliptical galaxy

Übergeordnetes Werk:	In: The Astrophysical Journal - IOP Publishing, 2022, 962(2024), 1, p 50
Übergeordnetes Werk:	volume:962 ; year:2024 ; number:1, p 50

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-4357/ad13ff

Katalog-ID:	DOAJ094813574

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allfields	10.3847/1538-4357/ad13ff doi (DE-627)DOAJ094813574 (DE-599)DOAJ6635069359c34b39a702013d4d0143f9 DE-627 ger DE-627 rakwb eng QB460-466 Kuria Watanabe verfasserin aut EMPRESS. XIII. Chemical Enrichment of Young Galaxies Near and Far at z ∼ 0 and 4–10: Fe/O, Ar/O, S/O, and N/O Measurements with a Comparison of Chemical Evolution Models 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present gas-phase elemental abundance ratios of thirteen local extremely metal-poor galaxies (EMPGs), including our new Keck/LRIS spectroscopy determinations together with 33 James Webb Space Telescope z ∼ 4–10 star-forming galaxies in the literature, and compare chemical evolution models. We develop chemical evolution models with the yields of core-collapse supernovae (CCSNe), Type Ia SNe, hypernovae (HNe), and pair-instability supernovae (PISNe), and compare the EMPGs and high- z galaxies in conjunction with dust depletion contributions. We find that high Fe/O values of EMPGs can (cannot) be explained by PISN metal enrichments (CCSN/HN enrichments even with the mixing-and-fallback mechanism enhancing iron abundance), while the observed Ar/O and S/O values are much smaller than the predictions of the PISN models. The abundance ratios of EMPGs can be explained by the combination of Type Ia SNe and CCSNe/HNe whose inner layers of argon and sulfur mostly fallback, which are comparable to the Sculptor stellar chemical abundance distribution, suggesting that early chemical enrichment has taken place in the EMPGs. Comparing our chemical evolution models with the star-forming galaxies at z ∼ 4–10, we find that the Ar/O and S/O ratios of the high- z galaxies are comparable to those of the CCSN/HN models, while the majority of high- z galaxies do not have constraints good enough to rule out contributions from PISNe. The high N/O ratio recently reported in GN-z11 cannot be explained even by rotating PISNe, but could be reproduced by the winds of rotating Wolf–Rayet stars that end up as a direct collapse. Galaxy chemical evolution Galaxy evolution Chemical enrichment Chemical abundances Galaxy formation Sculptor dwarf elliptical galaxy Astrophysics Masami Ouchi verfasserin aut Kimihiko Nakajima verfasserin aut Yuki Isobe verfasserin aut Nozomu Tominaga verfasserin aut Akihiro Suzuki verfasserin aut Miho N. Ishigaki verfasserin aut Ken’ichi Nomoto verfasserin aut Koh Takahashi verfasserin aut Yuichi Harikane verfasserin aut Shun Hatano verfasserin aut Haruka Kusakabe verfasserin aut Takashi J. Moriya verfasserin aut Moka Nishigaki verfasserin aut Yoshiaki Ono verfasserin aut Masato Onodera verfasserin aut Yuma Sugahara verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 962(2024), 1, p 50 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:962 year:2024 number:1, p 50 https://doi.org/10.3847/1538-4357/ad13ff kostenfrei https://doaj.org/article/6635069359c34b39a702013d4d0143f9 kostenfrei https://doi.org/10.3847/1538-4357/ad13ff kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 962 2024 1, p 50
spelling	10.3847/1538-4357/ad13ff doi (DE-627)DOAJ094813574 (DE-599)DOAJ6635069359c34b39a702013d4d0143f9 DE-627 ger DE-627 rakwb eng QB460-466 Kuria Watanabe verfasserin aut EMPRESS. XIII. Chemical Enrichment of Young Galaxies Near and Far at z ∼ 0 and 4–10: Fe/O, Ar/O, S/O, and N/O Measurements with a Comparison of Chemical Evolution Models 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present gas-phase elemental abundance ratios of thirteen local extremely metal-poor galaxies (EMPGs), including our new Keck/LRIS spectroscopy determinations together with 33 James Webb Space Telescope z ∼ 4–10 star-forming galaxies in the literature, and compare chemical evolution models. We develop chemical evolution models with the yields of core-collapse supernovae (CCSNe), Type Ia SNe, hypernovae (HNe), and pair-instability supernovae (PISNe), and compare the EMPGs and high- z galaxies in conjunction with dust depletion contributions. We find that high Fe/O values of EMPGs can (cannot) be explained by PISN metal enrichments (CCSN/HN enrichments even with the mixing-and-fallback mechanism enhancing iron abundance), while the observed Ar/O and S/O values are much smaller than the predictions of the PISN models. The abundance ratios of EMPGs can be explained by the combination of Type Ia SNe and CCSNe/HNe whose inner layers of argon and sulfur mostly fallback, which are comparable to the Sculptor stellar chemical abundance distribution, suggesting that early chemical enrichment has taken place in the EMPGs. Comparing our chemical evolution models with the star-forming galaxies at z ∼ 4–10, we find that the Ar/O and S/O ratios of the high- z galaxies are comparable to those of the CCSN/HN models, while the majority of high- z galaxies do not have constraints good enough to rule out contributions from PISNe. The high N/O ratio recently reported in GN-z11 cannot be explained even by rotating PISNe, but could be reproduced by the winds of rotating Wolf–Rayet stars that end up as a direct collapse. Galaxy chemical evolution Galaxy evolution Chemical enrichment Chemical abundances Galaxy formation Sculptor dwarf elliptical galaxy Astrophysics Masami Ouchi verfasserin aut Kimihiko Nakajima verfasserin aut Yuki Isobe verfasserin aut Nozomu Tominaga verfasserin aut Akihiro Suzuki verfasserin aut Miho N. Ishigaki verfasserin aut Ken’ichi Nomoto verfasserin aut Koh Takahashi verfasserin aut Yuichi Harikane verfasserin aut Shun Hatano verfasserin aut Haruka Kusakabe verfasserin aut Takashi J. Moriya verfasserin aut Moka Nishigaki verfasserin aut Yoshiaki Ono verfasserin aut Masato Onodera verfasserin aut Yuma Sugahara verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 962(2024), 1, p 50 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:962 year:2024 number:1, p 50 https://doi.org/10.3847/1538-4357/ad13ff kostenfrei https://doaj.org/article/6635069359c34b39a702013d4d0143f9 kostenfrei https://doi.org/10.3847/1538-4357/ad13ff kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 962 2024 1, p 50
allfields_unstemmed	10.3847/1538-4357/ad13ff doi (DE-627)DOAJ094813574 (DE-599)DOAJ6635069359c34b39a702013d4d0143f9 DE-627 ger DE-627 rakwb eng QB460-466 Kuria Watanabe verfasserin aut EMPRESS. XIII. Chemical Enrichment of Young Galaxies Near and Far at z ∼ 0 and 4–10: Fe/O, Ar/O, S/O, and N/O Measurements with a Comparison of Chemical Evolution Models 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present gas-phase elemental abundance ratios of thirteen local extremely metal-poor galaxies (EMPGs), including our new Keck/LRIS spectroscopy determinations together with 33 James Webb Space Telescope z ∼ 4–10 star-forming galaxies in the literature, and compare chemical evolution models. We develop chemical evolution models with the yields of core-collapse supernovae (CCSNe), Type Ia SNe, hypernovae (HNe), and pair-instability supernovae (PISNe), and compare the EMPGs and high- z galaxies in conjunction with dust depletion contributions. We find that high Fe/O values of EMPGs can (cannot) be explained by PISN metal enrichments (CCSN/HN enrichments even with the mixing-and-fallback mechanism enhancing iron abundance), while the observed Ar/O and S/O values are much smaller than the predictions of the PISN models. The abundance ratios of EMPGs can be explained by the combination of Type Ia SNe and CCSNe/HNe whose inner layers of argon and sulfur mostly fallback, which are comparable to the Sculptor stellar chemical abundance distribution, suggesting that early chemical enrichment has taken place in the EMPGs. Comparing our chemical evolution models with the star-forming galaxies at z ∼ 4–10, we find that the Ar/O and S/O ratios of the high- z galaxies are comparable to those of the CCSN/HN models, while the majority of high- z galaxies do not have constraints good enough to rule out contributions from PISNe. The high N/O ratio recently reported in GN-z11 cannot be explained even by rotating PISNe, but could be reproduced by the winds of rotating Wolf–Rayet stars that end up as a direct collapse. Galaxy chemical evolution Galaxy evolution Chemical enrichment Chemical abundances Galaxy formation Sculptor dwarf elliptical galaxy Astrophysics Masami Ouchi verfasserin aut Kimihiko Nakajima verfasserin aut Yuki Isobe verfasserin aut Nozomu Tominaga verfasserin aut Akihiro Suzuki verfasserin aut Miho N. Ishigaki verfasserin aut Ken’ichi Nomoto verfasserin aut Koh Takahashi verfasserin aut Yuichi Harikane verfasserin aut Shun Hatano verfasserin aut Haruka Kusakabe verfasserin aut Takashi J. Moriya verfasserin aut Moka Nishigaki verfasserin aut Yoshiaki Ono verfasserin aut Masato Onodera verfasserin aut Yuma Sugahara verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 962(2024), 1, p 50 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:962 year:2024 number:1, p 50 https://doi.org/10.3847/1538-4357/ad13ff kostenfrei https://doaj.org/article/6635069359c34b39a702013d4d0143f9 kostenfrei https://doi.org/10.3847/1538-4357/ad13ff kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 962 2024 1, p 50
allfieldsGer	10.3847/1538-4357/ad13ff doi (DE-627)DOAJ094813574 (DE-599)DOAJ6635069359c34b39a702013d4d0143f9 DE-627 ger DE-627 rakwb eng QB460-466 Kuria Watanabe verfasserin aut EMPRESS. XIII. Chemical Enrichment of Young Galaxies Near and Far at z ∼ 0 and 4–10: Fe/O, Ar/O, S/O, and N/O Measurements with a Comparison of Chemical Evolution Models 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present gas-phase elemental abundance ratios of thirteen local extremely metal-poor galaxies (EMPGs), including our new Keck/LRIS spectroscopy determinations together with 33 James Webb Space Telescope z ∼ 4–10 star-forming galaxies in the literature, and compare chemical evolution models. We develop chemical evolution models with the yields of core-collapse supernovae (CCSNe), Type Ia SNe, hypernovae (HNe), and pair-instability supernovae (PISNe), and compare the EMPGs and high- z galaxies in conjunction with dust depletion contributions. We find that high Fe/O values of EMPGs can (cannot) be explained by PISN metal enrichments (CCSN/HN enrichments even with the mixing-and-fallback mechanism enhancing iron abundance), while the observed Ar/O and S/O values are much smaller than the predictions of the PISN models. The abundance ratios of EMPGs can be explained by the combination of Type Ia SNe and CCSNe/HNe whose inner layers of argon and sulfur mostly fallback, which are comparable to the Sculptor stellar chemical abundance distribution, suggesting that early chemical enrichment has taken place in the EMPGs. Comparing our chemical evolution models with the star-forming galaxies at z ∼ 4–10, we find that the Ar/O and S/O ratios of the high- z galaxies are comparable to those of the CCSN/HN models, while the majority of high- z galaxies do not have constraints good enough to rule out contributions from PISNe. The high N/O ratio recently reported in GN-z11 cannot be explained even by rotating PISNe, but could be reproduced by the winds of rotating Wolf–Rayet stars that end up as a direct collapse. Galaxy chemical evolution Galaxy evolution Chemical enrichment Chemical abundances Galaxy formation Sculptor dwarf elliptical galaxy Astrophysics Masami Ouchi verfasserin aut Kimihiko Nakajima verfasserin aut Yuki Isobe verfasserin aut Nozomu Tominaga verfasserin aut Akihiro Suzuki verfasserin aut Miho N. Ishigaki verfasserin aut Ken’ichi Nomoto verfasserin aut Koh Takahashi verfasserin aut Yuichi Harikane verfasserin aut Shun Hatano verfasserin aut Haruka Kusakabe verfasserin aut Takashi J. Moriya verfasserin aut Moka Nishigaki verfasserin aut Yoshiaki Ono verfasserin aut Masato Onodera verfasserin aut Yuma Sugahara verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 962(2024), 1, p 50 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:962 year:2024 number:1, p 50 https://doi.org/10.3847/1538-4357/ad13ff kostenfrei https://doaj.org/article/6635069359c34b39a702013d4d0143f9 kostenfrei https://doi.org/10.3847/1538-4357/ad13ff kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 962 2024 1, p 50
allfieldsSound	10.3847/1538-4357/ad13ff doi (DE-627)DOAJ094813574 (DE-599)DOAJ6635069359c34b39a702013d4d0143f9 DE-627 ger DE-627 rakwb eng QB460-466 Kuria Watanabe verfasserin aut EMPRESS. XIII. Chemical Enrichment of Young Galaxies Near and Far at z ∼ 0 and 4–10: Fe/O, Ar/O, S/O, and N/O Measurements with a Comparison of Chemical Evolution Models 2024 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier We present gas-phase elemental abundance ratios of thirteen local extremely metal-poor galaxies (EMPGs), including our new Keck/LRIS spectroscopy determinations together with 33 James Webb Space Telescope z ∼ 4–10 star-forming galaxies in the literature, and compare chemical evolution models. We develop chemical evolution models with the yields of core-collapse supernovae (CCSNe), Type Ia SNe, hypernovae (HNe), and pair-instability supernovae (PISNe), and compare the EMPGs and high- z galaxies in conjunction with dust depletion contributions. We find that high Fe/O values of EMPGs can (cannot) be explained by PISN metal enrichments (CCSN/HN enrichments even with the mixing-and-fallback mechanism enhancing iron abundance), while the observed Ar/O and S/O values are much smaller than the predictions of the PISN models. The abundance ratios of EMPGs can be explained by the combination of Type Ia SNe and CCSNe/HNe whose inner layers of argon and sulfur mostly fallback, which are comparable to the Sculptor stellar chemical abundance distribution, suggesting that early chemical enrichment has taken place in the EMPGs. Comparing our chemical evolution models with the star-forming galaxies at z ∼ 4–10, we find that the Ar/O and S/O ratios of the high- z galaxies are comparable to those of the CCSN/HN models, while the majority of high- z galaxies do not have constraints good enough to rule out contributions from PISNe. The high N/O ratio recently reported in GN-z11 cannot be explained even by rotating PISNe, but could be reproduced by the winds of rotating Wolf–Rayet stars that end up as a direct collapse. Galaxy chemical evolution Galaxy evolution Chemical enrichment Chemical abundances Galaxy formation Sculptor dwarf elliptical galaxy Astrophysics Masami Ouchi verfasserin aut Kimihiko Nakajima verfasserin aut Yuki Isobe verfasserin aut Nozomu Tominaga verfasserin aut Akihiro Suzuki verfasserin aut Miho N. Ishigaki verfasserin aut Ken’ichi Nomoto verfasserin aut Koh Takahashi verfasserin aut Yuichi Harikane verfasserin aut Shun Hatano verfasserin aut Haruka Kusakabe verfasserin aut Takashi J. Moriya verfasserin aut Moka Nishigaki verfasserin aut Yoshiaki Ono verfasserin aut Masato Onodera verfasserin aut Yuma Sugahara verfasserin aut In The Astrophysical Journal IOP Publishing, 2022 962(2024), 1, p 50 (DE-627)269019219 (DE-600)1473835-1 15384357 nnns volume:962 year:2024 number:1, p 50 https://doi.org/10.3847/1538-4357/ad13ff kostenfrei https://doaj.org/article/6635069359c34b39a702013d4d0143f9 kostenfrei https://doi.org/10.3847/1538-4357/ad13ff kostenfrei https://doaj.org/toc/1538-4357 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_702 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 962 2024 1, p 50
language	English
source	In The Astrophysical Journal 962(2024), 1, p 50 volume:962 year:2024 number:1, p 50
sourceStr	In The Astrophysical Journal 962(2024), 1, p 50 volume:962 year:2024 number:1, p 50
format_phy_str_mv	Article
institution	findex.gbv.de
topic_facet	Galaxy chemical evolution Galaxy evolution Chemical enrichment Chemical abundances Galaxy formation Sculptor dwarf elliptical galaxy Astrophysics
isfreeaccess_bool	true
container_title	The Astrophysical Journal
authorswithroles_txt_mv	Kuria Watanabe @@aut@@ Masami Ouchi @@aut@@ Kimihiko Nakajima @@aut@@ Yuki Isobe @@aut@@ Nozomu Tominaga @@aut@@ Akihiro Suzuki @@aut@@ Miho N. Ishigaki @@aut@@ Ken’ichi Nomoto @@aut@@ Koh Takahashi @@aut@@ Yuichi Harikane @@aut@@ Shun Hatano @@aut@@ Haruka Kusakabe @@aut@@ Takashi J. Moriya @@aut@@ Moka Nishigaki @@aut@@ Yoshiaki Ono @@aut@@ Masato Onodera @@aut@@ Yuma Sugahara @@aut@@
publishDateDaySort_date	2024-01-01T00:00:00Z
hierarchy_top_id	269019219
id	DOAJ094813574
language_de	englisch
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callnumber-first	Q - Science
author	Kuria Watanabe
spellingShingle	Kuria Watanabe misc QB460-466 misc Galaxy chemical evolution misc Galaxy evolution misc Chemical enrichment misc Chemical abundances misc Galaxy formation misc Sculptor dwarf elliptical galaxy misc Astrophysics EMPRESS. XIII. Chemical Enrichment of Young Galaxies Near and Far at z ∼ 0 and 4–10: Fe/O, Ar/O, S/O, and N/O Measurements with a Comparison of Chemical Evolution Models
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topic_title	QB460-466 EMPRESS. XIII. Chemical Enrichment of Young Galaxies Near and Far at z ∼ 0 and 4–10: Fe/O, Ar/O, S/O, and N/O Measurements with a Comparison of Chemical Evolution Models Galaxy chemical evolution Galaxy evolution Chemical enrichment Chemical abundances Galaxy formation Sculptor dwarf elliptical galaxy
topic	misc QB460-466 misc Galaxy chemical evolution misc Galaxy evolution misc Chemical enrichment misc Chemical abundances misc Galaxy formation misc Sculptor dwarf elliptical galaxy misc Astrophysics
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title	EMPRESS. XIII. Chemical Enrichment of Young Galaxies Near and Far at z ∼ 0 and 4–10: Fe/O, Ar/O, S/O, and N/O Measurements with a Comparison of Chemical Evolution Models
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title_full	EMPRESS. XIII. Chemical Enrichment of Young Galaxies Near and Far at z ∼ 0 and 4–10: Fe/O, Ar/O, S/O, and N/O Measurements with a Comparison of Chemical Evolution Models
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author_browse	Kuria Watanabe Masami Ouchi Kimihiko Nakajima Yuki Isobe Nozomu Tominaga Akihiro Suzuki Miho N. Ishigaki Ken’ichi Nomoto Koh Takahashi Yuichi Harikane Shun Hatano Haruka Kusakabe Takashi J. Moriya Moka Nishigaki Yoshiaki Ono Masato Onodera Yuma Sugahara
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title_sort	empress. xiii. chemical enrichment of young galaxies near and far at z ∼ 0 and 4–10: fe/o, ar/o, s/o, and n/o measurements with a comparison of chemical evolution models
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title_auth	EMPRESS. XIII. Chemical Enrichment of Young Galaxies Near and Far at z ∼ 0 and 4–10: Fe/O, Ar/O, S/O, and N/O Measurements with a Comparison of Chemical Evolution Models
abstract	We present gas-phase elemental abundance ratios of thirteen local extremely metal-poor galaxies (EMPGs), including our new Keck/LRIS spectroscopy determinations together with 33 James Webb Space Telescope z ∼ 4–10 star-forming galaxies in the literature, and compare chemical evolution models. We develop chemical evolution models with the yields of core-collapse supernovae (CCSNe), Type Ia SNe, hypernovae (HNe), and pair-instability supernovae (PISNe), and compare the EMPGs and high- z galaxies in conjunction with dust depletion contributions. We find that high Fe/O values of EMPGs can (cannot) be explained by PISN metal enrichments (CCSN/HN enrichments even with the mixing-and-fallback mechanism enhancing iron abundance), while the observed Ar/O and S/O values are much smaller than the predictions of the PISN models. The abundance ratios of EMPGs can be explained by the combination of Type Ia SNe and CCSNe/HNe whose inner layers of argon and sulfur mostly fallback, which are comparable to the Sculptor stellar chemical abundance distribution, suggesting that early chemical enrichment has taken place in the EMPGs. Comparing our chemical evolution models with the star-forming galaxies at z ∼ 4–10, we find that the Ar/O and S/O ratios of the high- z galaxies are comparable to those of the CCSN/HN models, while the majority of high- z galaxies do not have constraints good enough to rule out contributions from PISNe. The high N/O ratio recently reported in GN-z11 cannot be explained even by rotating PISNe, but could be reproduced by the winds of rotating Wolf–Rayet stars that end up as a direct collapse.
abstractGer	We present gas-phase elemental abundance ratios of thirteen local extremely metal-poor galaxies (EMPGs), including our new Keck/LRIS spectroscopy determinations together with 33 James Webb Space Telescope z ∼ 4–10 star-forming galaxies in the literature, and compare chemical evolution models. We develop chemical evolution models with the yields of core-collapse supernovae (CCSNe), Type Ia SNe, hypernovae (HNe), and pair-instability supernovae (PISNe), and compare the EMPGs and high- z galaxies in conjunction with dust depletion contributions. We find that high Fe/O values of EMPGs can (cannot) be explained by PISN metal enrichments (CCSN/HN enrichments even with the mixing-and-fallback mechanism enhancing iron abundance), while the observed Ar/O and S/O values are much smaller than the predictions of the PISN models. The abundance ratios of EMPGs can be explained by the combination of Type Ia SNe and CCSNe/HNe whose inner layers of argon and sulfur mostly fallback, which are comparable to the Sculptor stellar chemical abundance distribution, suggesting that early chemical enrichment has taken place in the EMPGs. Comparing our chemical evolution models with the star-forming galaxies at z ∼ 4–10, we find that the Ar/O and S/O ratios of the high- z galaxies are comparable to those of the CCSN/HN models, while the majority of high- z galaxies do not have constraints good enough to rule out contributions from PISNe. The high N/O ratio recently reported in GN-z11 cannot be explained even by rotating PISNe, but could be reproduced by the winds of rotating Wolf–Rayet stars that end up as a direct collapse.
abstract_unstemmed	We present gas-phase elemental abundance ratios of thirteen local extremely metal-poor galaxies (EMPGs), including our new Keck/LRIS spectroscopy determinations together with 33 James Webb Space Telescope z ∼ 4–10 star-forming galaxies in the literature, and compare chemical evolution models. We develop chemical evolution models with the yields of core-collapse supernovae (CCSNe), Type Ia SNe, hypernovae (HNe), and pair-instability supernovae (PISNe), and compare the EMPGs and high- z galaxies in conjunction with dust depletion contributions. We find that high Fe/O values of EMPGs can (cannot) be explained by PISN metal enrichments (CCSN/HN enrichments even with the mixing-and-fallback mechanism enhancing iron abundance), while the observed Ar/O and S/O values are much smaller than the predictions of the PISN models. The abundance ratios of EMPGs can be explained by the combination of Type Ia SNe and CCSNe/HNe whose inner layers of argon and sulfur mostly fallback, which are comparable to the Sculptor stellar chemical abundance distribution, suggesting that early chemical enrichment has taken place in the EMPGs. Comparing our chemical evolution models with the star-forming galaxies at z ∼ 4–10, we find that the Ar/O and S/O ratios of the high- z galaxies are comparable to those of the CCSN/HN models, while the majority of high- z galaxies do not have constraints good enough to rule out contributions from PISNe. The high N/O ratio recently reported in GN-z11 cannot be explained even by rotating PISNe, but could be reproduced by the winds of rotating Wolf–Rayet stars that end up as a direct collapse.
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title_short	EMPRESS. XIII. Chemical Enrichment of Young Galaxies Near and Far at z ∼ 0 and 4–10: Fe/O, Ar/O, S/O, and N/O Measurements with a Comparison of Chemical Evolution Models
url	https://doi.org/10.3847/1538-4357/ad13ff https://doaj.org/article/6635069359c34b39a702013d4d0143f9 https://doaj.org/toc/1538-4357
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EMPRESS. XIII. Chemical Enrichment of Young Galaxies Near and Far at z ∼ 0 and 4–10: Fe/O, Ar/O, S/O, and N/O Measurements with a Comparison of Chemical Evolution Models

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